There are many public software packages that implement analytic methods for strong lens analysis. For example, lenstool [1]} and glafic [2]} provide specialised tools for cluster-scale lenses. For galaxy-galaxy lenses, dedicated software has been developed, such as gravlens [3]}, PixeLens [4]}, AutoLens [5]}, and Lenstronomy [6]}. Typical analytic functions include variations of power-law or cored profiles for the lensing mass, while more elaborate ensembles of basis functions like shapelets [7]}, [8]}, [9]}, [10]} can be used to capture the wider dynamic range of features often exhibited by high-redshift galaxies, especially when they are star-forming. While analytical methods are fast, they have two main disadvantages. First, complex light distributions like galaxies with resolved small-scale features or mergers are poorly modelled. Second, it requires lots of trial and error to infer the initial parameters describing the source shape, hence making it hard to automate these techniques.
